Table 3
Parameters and best-fit values used in modelling the SONG RV and RM data.
| Parameter | Symbol | Units | RV | RM |
|---|---|---|---|---|
| Epoch | Tp | BJD | 2457909.5906 (fixed) | 2457058.42722 ± 0.0003 |
| Period | P | d | 3.474119 (fixed) | 3.474135 (fixed) |
| Scaled semi-major axis | a∕R⋆ | – | – | 7.5 ± 0.04 |
| Planet-to-star ratio | p = Rp∕R⋆ | – | – | 0.1133 ± 0.0007 |
| Cosine of the inclination | cosi | – | – | 0.066 ± 0.002 |
| Eccentricity | e | – | 0 (fixed) | 0 (fixed) |
| RV amplitudea | K | km s−1 | 0 ± 600 | − 1000 ± 300 |
| Systemic velocitya | γ | km s−1 | − 21.3 ± 0.4 | − 21.07 ± 0.03 |
| RV jitter | σj | km s−1 |  |
– |
| Projected obliquity | λ | ^° | – | 0.6 ± 4 |
| Micro turbulence | ν | km s−1 | – | 2.0 ± 0.5 |
| Macro turbulence | ζ | km s−1 | – | 15.1 ± 0.6 |
| Projected rotation speed | vsini⋆ | km s−1 | – | 114 ± 3 |
| Limb darkening (SONG)b | u1 + u2 | – | – | 0.63 ± 0.01 |
| Limb darkening (IAC80)b | u1 + u2 | – | – | 0.42 ± 0.04 |
Notes. (a) Since the small phase coverage of the spectroscopic transit observations might cause short time-scale effects in the star, such as pulsations, to bias the observations we prefer the values for K and γ obtained from the RV modelling where such short time-scale effects are not coherent and included in the jitter term. (b) We employed Gaussian priors with a width of 0.05 on u1 + u2 using the appropriate limb-darkening coefficients from Claret & Bloemen (2011) for u1 + u2.
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